The Maria asteroid family - Sorbonne Université
Article Dans Une Revue Monthly Notices of the Royal Astronomical Society Année : 2017

The Maria asteroid family

V Carruba
  • Fonction : Auteur
J R Masiero
  • Fonction : Auteur
R C Domingos
  • Fonction : Auteur
M Huaman
  • Fonction : Auteur

Résumé

The Maria asteroid family is a group of S-type asteroids. Its location adjacent to the left side of the 3J:-1A mean-motion resonances could be the reason for the absence of the left side of the 'V' shape in the (a, 1/D) domain. This family can be considered as a likely source of ordinary chondrite-like material. In this work, we make use of the time dependence of the asymmetric coefficient A S describing the degree of asymmetry of the C distribution of a fictitious Maria family generated with the value of the ejection velocity parameter V EJ = 35 m s −1 to obtain an age estimate of 1750 −231 +537 Myr, in good agreement with the family age found in the literature. Analysing the contribution to the near-Earth object (NEO) population, we found that about 7.6 per cent of presently known near-Earth asteroids (NEAs) have orbits similar to asteroids from the Maria family. Only ∼1.7 per cent of our simulated family can stay in NEO space for more than 10 Myr, while only five asteroids become NEOs in the last 500 Myr of the simulation.
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Dates et versions

hal-02481200 , version 1 (17-02-2020)

Identifiants

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Safwan Aljbaae, V Carruba, J R Masiero, R C Domingos, M Huaman. The Maria asteroid family. Monthly Notices of the Royal Astronomical Society, 2017, 471 (4), pp.4820 - 4826. ⟨10.1093/mnras/stx1921⟩. ⟨hal-02481200⟩
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